The Origin of $r$-process Enhanced Metal-poor Halo Stars In Now-destroyed Ultra-faint Dwarf Galaxies

Brauer, Kaley; Ji, Alexander P.; Frebel, Anna; Dooley, Gregory A.; Gómez, Facundo A.; O’Shea, Brian W.

doi:10.3847/1538-4357/aafafb

Title: The Origin of $$r$$-process Enhanced Metal-poor Halo Stars In Now-destroyed Ultra-faint Dwarf Galaxies

Journal Article · Tue Feb 05 00:00:00 EST 2019 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/aafafb· OSTI ID:1613174

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^[3]; Gómez, Facundo A. ^[4];

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Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States); Joint Inst. for Nuclear Astrophysics - Center for the Evolution of the Elements (JINA-CEE) (United States)
Observatories of the Carnegie Inst. for Science, Pasadena, CA (United States); Joint Inst. for Nuclear Astrophysics - Center for the Evolution of the Elements (JINA-CEE) (United States)
Google, New York, NY (United States)
Univ. de La Serena (Chile)
Michigan State Univ., East Lansing, MI (United States); Joint Inst. for Nuclear Astrophysics - Center for the Evolution of the Elements (JINA-CEE) (United States)

The highly $$r$$-process-enhanced (r-II) metal-poor halo stars we observe today could play a key role in understanding early ultra-faint dwarf galaxies (UFDs), the smallest building blocks of the Milky Way. If a significant fraction of metal-poor r-II halo stars originated in the UFDs that merged to help form the Milky Way, observations of r-II stars could help us study these now-destroyed systems and probe the formation history of our Galaxy. To conduct our initial investigation into this possible connection, we use high-resolution cosmological simulations of Milky Way-mass galaxies from the Caterpillar suite in combination with a simple, empirically motivated treatment of $$r$$-process enrichment. Further, we determine the fraction of metal-poor halo stars that could have formed from highly $$r$$-process-enhanced gas in now-destroyed low-mass UFDs, the simulated r-II fraction, and compare it to the “as observed” r-II fraction. We find that the simulated fraction, $$f_{r-II,sim}$$ ~1%–2%, can account for around half of the “as observed” fraction, $$f_{r-II,obs}$$ ~ 2%–4%. The “as observed” fraction likely overrepresents the fraction of r-II stars due to incomplete sampling, though, meaning $$f_{r-II,sim}$$ likely accounts for more than half of the true fr-II,obs. Further considering some parameter variations and scatter between individual simulations, the simulated fraction can account for around 20%–80% of the “as observed” fraction.

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Research Organization:: Krell Institute, Ames, IA (United States)

Sponsoring Organization:: USDOE Office of Science (SC); Whiteman Fellowship; National Aeronautics and Space Administration (NASA); Space Telescope Science Institute; National Science Foundation (NSF); National Fund for Scientific and Technological Development (FONDECYT); Max Planck Society

Grant/Contract Number:: SC0019323; HST-HF2-51393.001; NAS5-26555; AST-1255160; AST-1716251; NNX15AP39G; 80NSSC18K1105; HSTAR-13261.01-A; AST-1514700; PHY-1430152

OSTI ID:: 1613174

Journal Information:: The Astrophysical Journal (Online), Vol. 871, Issue 2; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 20 works

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